The background due to GCRs can be computed using a convenient model, e.g., the force-field model with the corresponding local interstellar spectrum, considering explicitly the modulation potential [1]}, [2]}. The optimization can be performed over the set of model parameters \(n\)  by minimizing the difference between the modeled and measured NM responses using a convenient method [3]}, [4]}, [5]}, [6]}. The modeling of the global network NM response can be performed using the corresponding NM yield function, which establishes a connection between the primary CR flux at the top of the Earth's atmosphere and the count rate of the device. Since the secondary CRs, resulting from the primary CR induced cascade in the Earth's atmosphere, can reach the ground level and eventually be registered by a NM, the yield function incorporates the full complexity of the atmospheric cascade development including secondary particle propagation in the atmosphere and the efficiency of the detector itself to register the secondaries [7]}. The NM yield function can be determined by parameterization of experimental data, namely latitude survey(s) [8]}, [9]}, [10]} or can be assessed using Monte Carlo simulations of CR propagation in the atmosphere [11]}, [7]}. Recently, essential progress of Monte Carlo simulations of CR propagation in the atmosphere was achieved, which resulted in several newly computed NM functions [7]}, [14]}, [15]}, [16]}. A recently computed NM yield function by [15]}, [18]} is fully consistent with the experimental latitude surveys and was validated by achieving good agreement between model results and measurements, including space-borne data [19]}, [20]}, [21]}.
